This is a table of times of substorm onsets observed by IMAGE/FUV. The raw instrument counts in the FUV image with the greatest number of counts at time of onset, the X and Y pixel numbers for this greatest-count pixel, the onset geographic and geomagnetic latitude and longitude angles and local time, and the geocentric distance of IMAGE are also given for each onset.

This data set consists of images of thermospheric
O/N2 column density ratios at 2-min resolution during times of strong
geomagnetic storms (Dst.LT.-80nT) of 2000-2005. The ratios are generated
from dayside airglow observations of the IMAGE Far Ultraviolet (FUV)
Spectrographic Imager (SI). The SI has a peak response at the OI 135.6 nm
oxygen emission line and a bandpass of 131.0 to 140.0 nm which includes
the LBH band from N2 molecules. For each O/N2 plot, there is a plot of the
SI image from which the O/N2 plot was generated, and there is an IDL saveset
of the content of the O/N2 maps. The Information URL of this descriptor
identifies detailed discussions of the derivations of O/N2 rations from the
SI images.

This data set consists of images of thermospheric
O/N2 column density ratios at 2-min resolution during times of strong
geomagnetic storms (Dst.LT.-80nT) of 2000-2005. The ratios are generated
from dayside airglow observations of the IMAGE Far Ultraviolet (FUV)
Spectrographic Imager (SI). The SI has a peak response at the OI 135.6 nm
oxygen emission line and a bandpass of 131.0 to 140.0 nm which includes
the LBH band from N2 molecules. For each O/N2 plot, there is a plot of the
SI image from which the O/N2 plot was generated, and there is an IDL saveset
of the content of the O/N2 maps. The Information URL of this descriptor
identifies detailed discussions of the derivations of O/N2 rations from the
SI images.

This is a set of data at multiple processing levels from all IMAGE instruments. Built by a UNIX-afficionado requiring editing .cshrc's, etc., the data are in Universal Data Format (UDF), and at the moment, has no PC install documentation. UDF software is available to read the IMAGE UDF files.

Collection of RPI Daily Dynamic Spectrogram plots at NASA GSFC, covering complete mission period from 2000-04-21 to 2005-12-18. Dynamic Spectrograms present the time history of natural radio emissions in space between 3 and 1009 kHz while the IMAGE spacecraft orbits the Earth. This operating frequency range was selected by the RPI team to provide an optimal temporal resolution to the wave observations. Each image is a daily plot of the voltage spectral density of received signal (color scale) as function of operating frequency (vertical axis) and time (horizontal axis). Commonly used in the analysis of noise generators, spectral density is a frequency-dependent characteristic that describes how much power is generated by the emission source in a 1 Hz bandwidth. RPI Dynamic Spectograms plot a Voltage Spectral Density, which is root of power spectral density, measured in [V/root-Hz] units. Note that conversion of antenna voltage to electric field strength depends on effective length of receive antennas, and such conversion is not performed here. RPI is capable of detecting input radio emissions above its noise floor of 5 nV/root-Hz, which is determined by the internal white noise of the RPI antenna pre-amplifiers.

RPI passive wave measurement capturing voltage spectral density of the radio emissions in space as a function of frequency, typically between 3 and 1009 kHz. This operating frequency range was selected by the RPI team to provide optimal temporal resolution of the wave observations. Commonly used in the analysis of noise generators, spectral density is a frequency-dependent characteristic that describes how much power is generated by the emission source in a 1 Hz bandwidth. The original description of emissions was done in terms of thermal noise measurements, though the same approach also applies to non-thermal emissions such as AKR. CDF_DS_PT5M stores calibrated data from all three RPI antennas X, Y, and Z individually and a combined X+Y antenna channel. The data are presented as the Voltage Spectral Density (VSD), which is the root of power spectral density, measured in [V/root-Hz] units. Note that conversion of antenna voltage to electric field strength depends on the effective length of the receive antenna, and such conversion is not performed here. (See spase://SMWG/Instrument/IMAGE/RPI for a time history of the lengths of the three mutually orthogonal RPI dipole antennas.) RPI is capable of detecting input radio emissions above its noise floor of 5 nV/root-Hz, which is determined by the internal white noise of the RPI antenna pre-amplifiers. The VSD in RPI spectrogram data is presented in dB relative to 1 V/root-Hz (logarithmic scale), units of dB(V/root-Hz). The RPI instrument noise floor is 5 nV/root-Hz = -166 dB(V/root-Hz) at the receiver input. Software suggested by the science team for CDF file visualization: (1) Plotting tool at the CDAWeb portal, (2) For analysis beyond static image inspection, including color scale optimization, zooming, text export, alternative data representations in physical units, detailed frequency and time information, overlaid model fpe and fce graphs, and EPS quality figures, use BinBrowser software at UML, http://ulcar.uml.edu/rpi.html

RPI plasmagram full resolution data (received signal strength in the frequency-range frame), uncalibrated. Presented as instrument packets wrapped in the standard CCSDS headers. Description of the RPI instrument-level data model can be found at http://ulcar.uml.edu/RPI/RPITelemetryDataFormat_V2.8.pdf. Data are viewed/calibrated/edited by BinBrowser software, see http://ulcar.uml.edu/rpi.html for download and users' guide. RPI plasmagrams are visualized by plotting images in which received signal strength (color scale) is a function of echo delay (range in vertical scale) and radio-sounder frequency (horizontal scale) of the radar pulses. Echoes from important magnetospheric structures, such as the magnetopause and the plasmapause, appear as traces on plasmagrams. Plasmagram traces are intermixed with vertical signatures corresponding to the locally excited plasma resonances and various natural emissions propagating in space.

Collection of RPI Plasmagram images at University of Massachusetts Lowell, covering complete mission period from 2000-04-21 to 2005-12-18. Access to images is arranged via a webpage containing a query form with the time period of interest and options for search of expert-annotated plasmagrams. The query returns a list of qualifying plasmagrams with URLs pointing to images. RPI plasmagrams are visualized by plotting images in which received signal strength (color scale) is a function of echo delay (range in vertical scale) and radio-sounder frequency (horizontal scale) of the sounder pulses. Echoes that can be used to derive remote, long-range, magnetospheric electron-density profiles, appear as discrete traces on plasmagrams. These plasmagram traces are intermixed with vertical signatures with greater intensity at shorter ranges, corresponding to locally excited plasma resonances, and other vertical signatures that cover the entire listening period, i.e., the entire virtual-range scale, corresponding to various natural and/or man-made emissions propagating in space and/or local interference.

The electron density values listed in this file are derived from the IMAGE Radio
Plasma Imager (B.W. Reinisch, PI) data using an automatic fitting program
written by Phillip Webb with manual correction.
The electron number densities were produced using an automated procedure (with
manual correction when necessary) which attempted to self-consistently fit an
enhancement in the IMAGE RPI Dynamic Spectra to either 1) the Upper Hybrid
Resonance band, 2) the Z-mode or 3) the continuum edge. The automatic algorithm
works by rules determined by comparison of the active and passive RPI data
[Benson et al., GRL, vol. 31, L20803, doi:10.1029/2004GL020847, 2004].
The manual data points are not from frequencies chosen freely by a human. Rather
the human specifies that the computer should search for a peak or continuum edge
in a certain frequency region. Thus even the manual points are determined, in
part, by the automatic algorithms. Of course that does not guarantee that the
data points are right, but it does eliminate some human bias.

This set of daily plasmagrams/echograms comes from the IMAGE Radio Plasma Imager that studies the Earth's magnetophere in the 3 kHz to 3 MHz frequency range. RPI plasmagrams are visualized by plotting images in which received signal strength (color scale) is a function of echo delay (range in vertical scale) and radio-sounder frequency (horizontal scale) of the sounder pulses. Echoes that can be used to derive remote, long-range, magnetospheric electron-density profiles, appear as discrete traces on plasmagrams. These plasmagram traces are intermixed with vertical signatures with greater intensity at shorter ranges, corresponding to locally excited plasma resonances, and other vertical signatures that cover the entire listening period, i.e., the entire virtual-range scale, corresponding to various natural and/or man-made emissions propagating in space and/or local interference.

This data set contains calibrated level-2 images and spectra data from the Interface Region Imaging Spectrograph (IRIS).
UV images from IRIS telesccope record observations of features as small as 240 km (150 miles) on the sun every five to ten seconds at specific temperatures, ranging from 5,000 K and 65,000 K (and up to 10 million K during solar flares). This range is tailored to observe material traveling on the surface of the sun, called the photosphere, and in the lowermost layers of the atmosphere, called the chromosphere and transition region.
Spectra are obtained every one to two seconds along a slit (1/3 arcsec wide) of solar material at temperatures from 5,000 K to 10 million K, providing information on exactly how much light is visible from any specific wavelength. This corresponds to how much material is present at specific velociites, temperatures and densities.
The level-2 data is corrected for dark current, flat-field, and geometric deformation, scaled to the same plate-scale, and packaged into timeseries of slitjaw images and spectral raster scans. The calibration is preliminary and will improve in the coming months.